Physics
Scientific paper
Feb 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..555..226t&link_type=abstract
Cosmology and Particle Physics: CAPP 2000. AIP Conference Proceedings, Volume 555, pp. 226-242 (2001).
Physics
3
Observational Cosmology, Distances, Parallaxes, Distances, Redshifts, Radial Velocities, Spatial Distribution Of Galaxies, Supernovae
Scientific paper
The most secure route for the determination of H0 over scales out to ~30 000 km s-1 is provided by blue SNe Ia. They are nearly perfect standard candles with luminosity scatter of 0 dotmin 1 (after small corrections for differences in decline rate and color) as demonstrated by their exceptionally tight Hubble diagram (in B, V, and I). Inserting the absolute magnitude MB,V,I of SNeIa, which is fixed by eight SNeIa in galaxies with known Cepheid distances, yields H0=58.5+/-6.3 (2 sigma). Brightest cluster members, TF distances, and Dn-σ distances can be used to construct Hubble diagrams of clusters of galaxies. They have larger scatter than SNeIa, but are still useful. The Hubble diagrams can be calibrated by the Virgo, Fornax, and Coma clusters, respectively, whose distances are well determined by Cepheids, SNeIa, the TF relation and other less secure methods. The mean result from four cluster Hubble diagrams is H0=59+/-3 (+/-6 for systematic errors) over scales of >~10 000 km s-1. The above SNeIa lie predominantly in field galaxies. Other methods can be used to determine distances of field galaxies, like the TF or Dn-σ relations, but their larger intrinsic scatter invites severe selection effects (Malmquist bias) which limits their range to <=8000 km s-1. A literature compilation of H0 determinations, which are carefully corrected for selection effects, suggests H0=55+/-6. Of the several physical methods to determine distances and H0, the lensed quasar PG1115-080 gives the most significant result at present, i.e. H0<60. .
Reindl B.
Tammann Gustav A.
Thim Frank
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